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MITP Scientific Program Jets, particle production and transport - - PowerPoint PPT Presentation

Sep 04, 2023 591 likes •1.27k views

etc. Axions and defects in the early Universe Frank Steffen Theory Group Max Planck Institute for Physics Munich, Germany MITP Scientific Program Jets, particle production and transport properties in collider and cosmological environments

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SLIDE 1

Dark Matter in Cosmology and at Colliders

Axions and defects in the early Universe

MITP Scientific Program

Jets, particle production and transport properties in collider and cosmological environments

Mainz, July 28, 2014

Theory Group Max Planck Institute for Physics Munich, Germany

1

Frank Steffen etc.

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SLIDE 2

Dark Matter in Cosmology and at Colliders

LHC CERN

Geneva

Astroparticle Physics

What are the fundamental constituents of matter? What is the energy budget

  • f the Universe?

largest scales Cosmology smallest scales Particle Physics Standard Model

Planck

ESA

68% 27% 5%

standard particles dark energy

dark matter

What is the particle identity and origin

  • f dark matter?

mH=126 GeV

2

slide-3
SLIDE 3

Dark Matter in Cosmology and at Colliders

Particle Physics

  • 2012: LHC Higgs-boson discovery
  • Intrinsic fine tuning problems

? Hierarchy Problem (mH << MPlanck)

? Strong CP Problem (ΘQCD << 1) ? Small Neutrino Masses (mν << mH)

mH = 126 GeV

➔ Physics beyond the Standard Model Cosmology

68% 27% 5%

Standard particles dark energy

dark matter

  • 2013: Planck CMB sky map
  • Cosmological puzzles

? Matter-Antimatter Asymmetry

? Particle Identity & Origin of Dark Matter ? Dark Energy = Cosmological Constant

3

slide-4
SLIDE 4
  • stable or lifetime well above

the age of our Universe

  • electrically neutral
  • clusters
  • cold / warm
  • dissipationless
  • color neutral

Properties of Dark Matter

slide-5
SLIDE 5

Steffen Axions etc.

Dark matter ➔ Particle Identity of Dark Matter

galaxies - rotation velocities galaxy clusters - gravitational lensing large scale structure

68% 27% 5%

standard particles dark energy

dark matter

slide-6
SLIDE 6

Steffen Axions etc.

Dark Matter Candidates

WIMP - Weakly Interacting Massive Particle EWIP - Extremely Weakly Interacting Particle WIMP miracle axion condensate thermally produced EWIP DM

(1) (2) (3)

freeze out m/Tf ~ 20 eq. $DM! 0.2 pb "anni "anni ! 1 pb leads to the correct dark matter abundance. Fermi-scale annihilation cross section

6

QCD processes in the hot early Universe

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SLIDE 7

Steffen Axions etc.

TD >> T: X is never in th. eq. with the prim. plasma but thermally produced

7

Cosmic Relic Abundances

  • TR > TD: 1+2 3+X
  • TR > TD: 1+2 3+X

T > TD: X in thermal eq. with the primordial plasma T ~ TD: X decouples as a thermal relic Boltzmann eq. collision term

decoupling temp. of X reheating temp.

  • B. eq.)

(

slide-8
SLIDE 8

Steffen Axions etc.

Thermal EWIP DM production in the hot early Universe

☺

Image credit: Rhys Taylor, Cardiff University

  • e

+ e τ decay analysis: m

ga gb gc a gc

e G

gravitino ? TR = 109 GeV ? initial temperature

dark matter

68% 27% 5%

standard particles dark energy

G

~

G

~

today

7

QCD

slide-9
SLIDE 9

Steffen Axions etc. 9

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

1 GeV

CνB CMB

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axion Production

a

gb ga a gc

)

Axion Condensate

Axion Dark Matter

QCD

slide-10
SLIDE 10

Steffen Axions etc.

electroweak Supersymmetry Standard Model & Gravity graviton

G

extremely weak

neutralino WIMP

Supergravity gravitino EWIP

G

~

strong

Dark Matter Candidates

standard particles interactions superpartners Peccei-Quinn (PQ) Symmetry

a

axion EWIP

a

~

axino EWIP

10

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SLIDE 11

Steffen Axions etc. 11

Gauge Couplings Gaugino Mass Parameters

100 100000. 1.10 8 1.10 11 1.10 14 1.2 1.1 1 0.9 0.8 0.7 0.6 0.5 100 100000. 1.10 8 1.10 11 1.10 14 1.2 1.1 1 0.9 0.8 0.7 0.6 0.5

Q [GeV] 102 106 108 1011 1014 MGUT 1.2 1.1 1 0.9 0.8 0.7 0.6 0.5

  • 5/3 g(Q)

g(Q) gs(Q)

100 100000. 1.10 8 1.10 11 1.10 14 200 400 600 800 1000 100 100000. 1.10 8 1.10 11 1.10 14

Mα [GeV] Q [GeV] m1/2 = 400 GeV 102 106 108 1011 1014 MGUT 1000 800 600 400 200 M1(Q) M2(Q) M3(Q) M1(Q)/x1 M2(Q)/x2

Gauge Coupling Unification at MGUT 2 × 1016 GeV

(Super-) Gravity Dark Matter Hierarchy Stabilization Gauge Coupling Unification Consistent String Theory Extension of Space-Time Symmetry

Why Supersymmetry?

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SLIDE 12

Steffen Axions etc.

Conservation of R-Parity

  • superpotential:

WMSSM ← W∆L + W∆B

  • non-observation of L & B violating processes (proton stability, ...)
  • postulate conservation of R-Parity ← multiplicative quantum number

PR = (−1)3(B−L)+S =    +1 for SM, Hu, Hd −1 for

  • X ← superpartners

The lightest supersymmetric particle (LSP) is stable!!!

SM1 SUSY SM2

R-Parity

SM SUSY1 SUSY2

R-Parity

12

2

R-Parity Conservation

slide-13
SLIDE 13

Steffen Axions etc.

electroweak Supersymmetry Standard Model & Gravity graviton

G

extremely weak

neutralino WIMP

Supergravity gravitino EWIP

G

~

strong

Dark Matter Candidates

standard particles interactions superpartners Peccei-Quinn (PQ) Symmetry

a

axion EWIP

a

~

axino EWIP

13

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SLIDE 14

Steffen Axions etc. 14

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp. 400.000 y CMB LSS CνB

Standard Thermal History of the Universe

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SLIDE 15

Steffen Axions etc. 14

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

Supersymmetric Dark Matter in Cosmology and at Colliders

neutralino pair annihilation e χ0

1 e

χ0

1 → SM1 SM2

  • direct detection (CRESST, EDELWEISS, ...)

elastic neutralino scattering e χ0

1 A → e

χ0

1 A

  • prod.@colliders (Tevatron, LHC, ILC, ...)

neutralino pair production p p → e χ0

1 e

χ0

1 ... (Tevatron, LHC)

e+ e− → e χ0

1 e

χ0

1 ... (ILC)

[Talk by Manuel Drees]

18

[... , Jungman, Kamionkowski, Griest, ’96, ...]

6!7 6E7 6L7

Cold Thermal Relic

freeze out m/Tf ~ 20 eq.

10 GeV

WIMP freeze

  • ut

TR= ?

reheating temp. 400.000 y CMB LSS CνB

Standard Thermal History of the Universe

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SLIDE 16

Steffen Axions etc.

[Battaglia]

15

focus point region bulk region annihilation funnel coannihilation region

[see Baltz, Battaglia, Peskin, Wizansky, ’06]

Neutralino LSP Case

no colored sparticles involved

N

slide-17
SLIDE 17

Steffen Axions etc.

  • indirect detection (EGRET, GLAST, ...)

neutralino pair annihilation e χ0

1 e

χ0

1 → SM1 SM2

  • direct detection (CRESST, EDELWEISS, ...)

elastic neutralino scattering e χ0

1 A → e

χ0

1 A

  • prod.@colliders (Tevatron, LHC, ILC, ...)

neutralino pair production p p → e χ0

1 e

χ0

1 ... (Tevatron, LHC)

e+ e− → e χ0

1 e

χ0

1 ... (ILC)

[Talk by Manuel Drees]

Neutralino Neutralino energetische kosmische Strahlung

[a] [b] [c] [f] [e]

Neutralino

Atomkern

Wärme Rückstoß Proton Proton Neutralino Neutralino Standard- modell- teilchen

MAGIC ATLAS

[d]

CRESST

WIMP paradigm & prospects

DM-SM mediators

SM states DM states

Cosmological (also galactic) annihilation Collider WIMP pair-production WIMP-nucleus scattering

WIMP paradigm

16

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SLIDE 18

Steffen Axions etc. 17

High PT jet [ diff i l ] DM [mass difference is large] The pT of jets and leptons depend on the sparticle masses which are given by Colored particles get produced and decay into weakly interacting stable masses which are given by models DM weakly interacting stable particles R-parity conserving

Th i l j t + l t + i i E

(or l+l-, τ+τ−) High PT jet

The signal : jets + leptons + missing ET

[from B. Dutta’s Talk, SUSY 2007]

Neutralino DM Production at the LHC

SM Particles SM Particles Neutralino Neutralino

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SLIDE 19

Steffen Axions etc. 18

Collider Dark Matter Searches: Limits Only

M0' M1/2'

  • 2012 8TeV

5.8fb-1 2011 7TeV 4.7fb-1 Msquark' Mgluino'

  • 2011 7TeV

4.7fb-1 2012 8TeV 5.8fb-1

slide-20
SLIDE 20

Steffen Axions etc.

m ˜

χ0

1 (GeV)

log10 h R × σSI

˜ χ0

1p

  • cm2i

DAMA/Na DAMA/I CRESST-II (2012) EDELWEISS (2012) CDMS (2011) CoGeNT S I M P L E ( 2 1 2 ) C O U P P ( 2 1 2 ) Z E P L I N

  • I

I I ( 2 1 2 ) X E N O N 1 ( 2 1 1 ) XENON100 (2012) Observed Limit (90% CL) ±1 σ Expected ±1 σ Expected SuperCDMS1T (Projection) XENON1T (Projection)

mSUGRA

mh0 = 125.3 ± 0.6 GeV

10

1

10

2

10

3

−47 −46 −45 −44 −43 −42 −41 −40 −39

  • S. Akula, PN, arXiv:1210.0520 [hep-ph]. .

Direct neutralino WIMP dark matter searches

[Akula, Nath, arXiv:1210.0520]

19

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SLIDE 21

Steffen Axions etc. 20

[GeV]

4l

m 80 100 120 140 160 Events/2.5 GeV 5 10 15 20 25 30

  • 1

Ldt = 4.6 fb

∫

= 7 TeV: s

  • 1

Ldt = 20.7 fb

∫

= 8 TeV: s

4l →

(*)

ZZ → H

Data

(*)

Background ZZ t Background Z+jets, t =125 GeV)

H

Signal (m Syst.Unc.

Preliminary ATLAS [GeV]

4l

m

80 100 120 140 160 180

Events / 3 GeV

5 10 15 20 25 30 35

Data Z+X ,ZZ

*

γ Z =126 GeV

H

m

CMS Preliminary

  • 1

= 8 TeV, L = 19.6 fb s ;

  • 1

= 7 TeV, L = 5.1 fb s

Higgs discovery ! very impressive !

slide-22
SLIDE 22

Steffen Axions etc. 21

ATLAS

) µ Signal strength (

  • 1

+1

Combined 4l →

(*)

ZZ → H γ γ → H ν l ν l →

(*)

WW → H τ τ → H bb → W,Z H

  • 1

Ldt = 4.6 - 4.8 fb

∫

= 7 TeV: s

  • 1

Ldt = 13 - 20.7 fb

∫

= 8 TeV: s

  • 1

Ldt = 4.6 fb

∫

= 7 TeV: s

  • 1

Ldt = 20.7 fb

∫

= 8 TeV: s

  • 1

Ldt = 4.8 fb

∫

= 7 TeV: s

  • 1

Ldt = 20.7 fb

∫

= 8 TeV: s

  • 1

Ldt = 4.6 fb

∫

= 7 TeV: s

  • 1

Ldt = 20.7 fb

∫

= 8 TeV: s

  • 1

Ldt = 4.6 fb

∫

= 7 TeV: s

  • 1

Ldt = 13 fb

∫

= 8 TeV: s

  • 1

Ldt = 4.7 fb

∫

= 7 TeV: s

  • 1

Ldt = 13 fb

∫

= 8 TeV: s

= 125.5 GeV

H

m

0.20 ± = 1.30 µ

ATLAS Preliminary

ATLAS-CONF-2013-034 note: bb and ττ have been updated to full 2012 dataset (recently)

CMS

SM

σ / σ Best fit

0.5 1 1.5 2 2.5

0.28 ± = 0.92 µ

ZZ → H

0.20 ± = 0.68 µ

WW → H

0.27 ± = 0.77 µ

γ γ → H

0.41 ± = 1.10 µ

τ τ → H

0.62 ± = 1.15 µ

bb → H

0.14 ± = 0.80 µ

Combined

  • 1

19.6 fb ≤ = 8 TeV, L s

  • 1

5.1 fb ≤ = 7 TeV, L s

CMS Preliminary

= 0.65

SM

p

= 125.7 GeV

H

m

CMS-PAS-HIG-13-005

Higgs discovery Signal strengths & Standard Model expectations

slide-23
SLIDE 23

Steffen Axions etc. 22

100 1000 1500 1000 2000

114 114 114 1 1 4 114 1 1 4 118 118 1 1 8 1 1 8 1 1 8 118 119 119 119 119 1 1 9 119 1 2 120 120 120 122 122

100 1000 1500 1000 2000

m0 (GeV) m1/2 (GeV)

mh = 124 GeV

119 GeV 122.5 GeV 125 GeV 14 Ge 1 V

tan β = 10, A0 = 2.5 m0, µ > 0

100 1000 1500 1000 2000

114 114 114 114 1 1 4 114 1 1 4 118 118 1 1 8 118 118 118 118 119 1 1 9 1 1 9 119 119 119 120 120 120 120 120 1 2 2 1 2 2 122 122 124 124 1 2 5

100 1000 1500 1000 2000

m0 (GeV) m1/2 (GeV)

tan β = 40, A0 = 2.5 m0, µ > 0

1.3 1.5 1.65

126 GeV

mh = 125 GeV

124 GeV 122.5 GeV 119 GeV

g − 2

b → sγ exclusion

No ET signal

Bs → µ+µ− 95% CL

Stau co-annihilation

Constrained MSSM

[hep-ph]]

  • sparticle searches
  • (g-2)μ anomaly
  • mh contours
slide-24
SLIDE 24

Steffen Axions etc. 23

mH

mH=126 GeV ? Big Desert ? Standard Model after the Higgs discovery ? new physics ?

slide-25
SLIDE 25

Steffen Axions etc. 24

electroweak Supersymmetry Standard Model & Gravity graviton

G

extremely weak

neutralino WIMP

Supergravity gravitino EWIP

G

~

strong

New Class ➔ Extremely Weakly Interacting Particles (EWIPs)

Dark Matter Candidates

standard particles interactions superpartners Peccei-Quinn (PQ) Symmetry

a

axion EWIP

a

~

axino EWIP MPl=2.4 x1018 GeV

∝(p/MPl)n

∝(p/MW)n

MW~102 GeV

∝(p/fPQ)n

fPQ >109 GeV

σ

saxion EWIP

slide-26
SLIDE 26

Steffen Axions etc. 25

The general supergravity Lagrangian (N = 1, d = 4)

1 e L = − M2

P

2 R + gij∗ DµφiDµφ∗j − 1 2 g2 (Ref)−1ab DaDb +igij∗ χj

LγµDµχi L + εµνρσψLµγνDρψLσ

− 1 4 RefabF a

µνF b,µν +

1 8 εµνρσImfabF a

µνF b ρσ

+ i 2 RefabλaγµDµλb − e−1 1 2 ImfabDµ

  • eλa

Rγµλb R

  • +
  • −

√ 2g∂iDaλaχi

L +

1 4 √ 2g

  • (Ref)−1ab ∂ifbcDaλcχi

L

+ i 16 √ 2∂ifabλa[γµ, γν]χi

LF b µν −

1 2MP gDaλa

Rγµψµ

− i 2MP √ 2gij∗ Dµφ∗jψνγµγνχi

L + h.c.

  • −

i 8MP Refabψµ[γm, γn]γµλaF a

mn

−eK/2M2

P

  • 1

4M2

P

W ∗ψRµ[γµ, γν]ψLν + 1 2MP √ 2DiW ψµγµχi

L

+ 1 2 DiDjW χ c

L iχj L +

1 4 gij∗ Dj∗ W ∗∂ifabλa

Rλb L + h.c.

  • −eK/M2

P

  • gij∗

(DiW )

  • Dj∗ W ∗

− 3 |W |2 M2

P

  • + O(M−2

P

) .

gravitino Planck scale

gaugino gauge boson

The Supergravity Lagrangian (N=1, d=4)

[Cremmer, Ferrara, Girardello, Van Proeyen, ’83]

Supergravity (N=1, d=4)

slide-27
SLIDE 27

Steffen Axions etc. 26

Supersymmetric Hadronic Axion Model

Lint

PQ =

↵s 8⇡fPQ 

  • Gb µνGb

µν 2DbDb 2i¯

˜ gb

MµDµ˜

gb

M

  • + a

⇣ Gb µν e Gb

µν + 2¯

˜ gb

Mµ5Dµ˜

gb

M

⌘ i¯ ˜ aM [µ, ν] 2 5˜ gb

MGb µν + 2¯

˜ aMDb˜ gb

M

  • , (8)

Lint

PQ =

p 2↵s 8⇡fPQ Z d2✓A W bW b + h.c.

erfield A = ( + ia)/ p 2 + p 2✓˜ a + FA✓✓, w

teractions of A with the color-field-str W b = ˜ gb + Db✓ µν✓Gb

µν + i✓✓µDµ¯

˜ gb

Peccei-Quinn (PQ) scale saxion axion axino

[ ..., Graf, Steffen, JCAP , 2013]

gluino gluon

d Db = gs P

˜ q ˜

q∗tb˜ q

squark

d ↵s = g2

s/4⇡.

PQ field strength

slide-28
SLIDE 28

Steffen Axions etc. 27

Supersymmetric Hadronic (KSVZ) Axion Model

a Q ˜ gb ˜ ga Q ˜ Q

˜ ga ˜ gc gb a Q Q Q ˜ Q

a Q gb ga

KSVZ [Kim ’79; Shifman, Vainshtein,Zakharov ’80]

heavy KSVZ (s)quark loops

slide-29
SLIDE 29

Steffen Axions etc. 28 fa ma 1012 109 106 103 eV meV eV keV

Telescope

Laboratory Excess radiation Hot DM Globular cluster stars (photons) GC stars & White dwarf cooling

  • (electrons)

Too many events SN 1987A Burst duration Cold DM ADMX

CAST

GeV

Astrophysical Axion Bounds Bounds from Axion Searches Cosmological Axion Bounds

ma 0.6 meV (1010 GeV/fPQ)

Axion Mass Peccei-Quinn Scale

t fa 6 × 108 GeV

Constraints on the Peccei-Quinn (PQ) scale fPQ

slide-30
SLIDE 30

Steffen Axions etc.

Extremely Weakly Interacting Particles (EWIPs)

galaxies - rotation velocities galaxy clusters - gravitational lensing large scale structure

☺ well-motivated candidates for dark matter ☺

68% 27% 5%

standard particles dark energy

gravitino

G

~

axion

a

axino

a

~

New Physics Origin

dark matter

EWIPs ???

5 29

slide-31
SLIDE 31

Steffen Axions etc. 30

High Reheating Temperature Scenarios

68% 27% 5%

standard particles

radiation dominated

  • mat. dom.

Λ dom. today 1eV 1 MeV inflation

? TR= 109 GeV ?

time Thermal Leptogenesis

requires TR > 109 GeV ➔ baryon asymmetry Big Bang Nucleosynthesis reheating temperature

slide-32
SLIDE 32

Steffen Axions etc. 31

High Reheating Temperature Scenarios

68% 27% 5%

standard particles

  • e

+ e τ decay analysis: m

ga gb gc a gc

e G

radiation dominated

  • mat. dom.

Λ dom. today 1eV 1 MeV inflation

? TR= 109 GeV ?

time Thermal EWIP production Thermal Leptogenesis

EWIP

∝ (p/MPl)n ∝ (TR/MPl)n

requires TR > 109 GeV ➔ baryon asymmetry

dark matter

stable & non-relativ.

Big Bang Nucleosynthesis reheating temperature

slide-33
SLIDE 33

Steffen Axions etc.

TD >> T: X is never in th. eq. with the prim. plasma but thermally produced

32

Cosmic Relic Abundances

  • TR > TD: 1+2 3+X
  • TR > TD: 1+2 3+X

T > TD: X in thermal eq. with the primordial plasma T ~ TD: X decouples as a hot thermal relic Boltzmann eq. collision term

decoupling temp. of X reheating temp.

slide-34
SLIDE 34

Steffen Axions etc. 33

Calculation of the Collsion Term

Process A: ga + gb → gc + a + gb ga gc a + gb ga a gc ga gb gc a + gb ga gc a Process B: qi + ¯ qj → ga + a qi ¯ qj a ga Process C: qi + ga → qj + a (crossing of B)

  • Hard Part: k > kcut
  • Soft Part: k < kcut

[cf. Braaten, Yuan, ’91]

  • Thermal Production Rate of X
  • Hard Thermal Loop (HTL) Resummation

g a a g

slide-35
SLIDE 35

Steffen Axions etc. 34

Thermal Axion Production in the Hot QGP

[Masso et al., ’02; Sikivie, ’08; Graf, FDS, ’10]

TD ≈ 9.6 × 106 GeV

  • fPQ

1010 GeV 2.246

Axion Decoupling Temperature

[Graf, FDS,1008.4528]

Process A: ga + gb → gc + a

+ gb ga gc a + gb ga a gc ga gb gc a + gb ga gc a

Process B: qi + ¯ qj → ga + a qi ¯ qj a ga Process C: qi + ga → qj + a (crossing of B)

10

4

10

6

10

8

10

10

10

12

10

  • 8

10

  • 6

10

  • 4

10

  • 2

g a a g

Hard Part Soft Part Axion Yield

[Graf, FDS, arXiv:1008.4528]

slide-36
SLIDE 36

Steffen Axions etc. 35

Axion Dark Matter

10

8

10

9

10

10

10

11

10

12

10

  • 10

10

  • 8

10

  • 6

10

  • 4

10

  • 2

1

[Graf, FDS, arXiv:1008.4528]

ma 0.6 meV (1010 GeV/fPQ)

Axion Mass Axion Condensate: CDM

y ΩMIS

a

h2 ∼ 0.15 θ2

i (fPQ/1012 GeV)7/6

[... , Sikivie, ’08; Kim, Carosi, ’08, ...]

slide-37
SLIDE 37

Steffen Axions etc. 35

Axion Dark Matter

10

8

10

9

10

10

10

11

10

12

10

  • 10

10

  • 8

10

  • 6

10

  • 4

10

  • 2

1

[Graf, FDS, arXiv:1008.4528]

ma 0.6 meV (1010 GeV/fPQ)

Axion Mass Thermal Axions: WDM/HDM

ΩTP/eq

a

h2

  • pa,02 + m2

a Y TP/eq a

s(T0)h2/ρc

18.6g6

s ln

1.501 gs 1010 GeV fPQ

  • 2

TR 1010 GeV

  • [Graf, FDS, arXiv:1008.4528]

Axion Condensate: CDM

y ΩMIS

a

h2 ∼ 0.15 θ2

i (fPQ/1012 GeV)7/6

[... , Sikivie, ’08; Kim, Carosi, ’08, ...]

slide-38
SLIDE 38

Steffen Axions etc. 35

Axion Dark Matter

10

8

10

9

10

10

10

11

10

12

10

  • 10

10

  • 8

10

  • 6

10

  • 4

10

  • 2

1

[Graf, FDS, arXiv:1008.4528]

ma 0.6 meV (1010 GeV/fPQ)

Axion Mass Thermal Axions: WDM/HDM

ΩTP/eq

a

h2

  • pa,02 + m2

a Y TP/eq a

s(T0)h2/ρc

18.6g6

s ln

1.501 gs 1010 GeV fPQ

  • 2

TR 1010 GeV

  • [Graf, FDS, arXiv:1008.4528]

[Masso et al., ’02; Sikivie, ’08; Graf, FDS, ’10]

TD ≈ 9.6 × 106 GeV

  • fPQ

1010 GeV 2.246

Axion Decoupling Temperature Axion Condensate: CDM

y ΩMIS

a

h2 ∼ 0.15 θ2

i (fPQ/1012 GeV)7/6

[... , Sikivie, ’08; Kim, Carosi, ’08, ...]

slide-39
SLIDE 39

Steffen Axions etc. 36

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

1 GeV

CνB CMB

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axion Production

a

gb ga a gc

)

Axion Condensate

Axion Dark Matter

QCD

slide-40
SLIDE 40

Steffen Axions etc. 37

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axino/ Gravitino Production

10 GeV

WIMP freeze

  • ut

Axino Dark Matter

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?), ...

  • [Covi, Kim, Roszkowski, ’99]

freeze out m/Tf ~ 20

eq.

NLSP T < 10 GeV NLSP ! LSP + SM

slide-41
SLIDE 41

Steffen Axions etc. 38

Axino LSP Case

Thermal G Production

  • τ NLSP →

G + τ

10 20 50 100 200 500 1000 100 200 500 1000 2000 5000 10 20 50 100 200 500 1000 100 200 500 1000 2000 5000

[...; Bolz, Brandenburg, Buchm¨ uller, ’01] [Pradler, FDS, ’06] [... ; Borgani, Masiero, Yamaguchi, ’96; ...] [... ; Covi, Kim, Roszkowski, ’99; ...]

10

!6

10

!4

10

!2

10

4

10

5

10

6

10

7

10

8

10

9

CDM ←(m˜

a, TR)≈(100 keV, 106 GeV)

HDM ←(m˜

a, TR)≈(100 eV , 109 GeV)

[ ... ; Brandenburg, FDS, ’04]

a a

a

[Brandenburg, FDS, ‘04]

see also [Covi et al., ’01]

identical to the gravitino case

and [Strumia, ’10]

slide-42
SLIDE 42

Steffen Axions etc. 38

Axino LSP Case

Thermal G Production

  • τ NLSP →

G + τ

10 20 50 100 200 500 1000 100 200 500 1000 2000 5000 10 20 50 100 200 500 1000 100 200 500 1000 2000 5000

[...; Bolz, Brandenburg, Buchm¨ uller, ’01] [Pradler, FDS, ’06] [... ; Borgani, Masiero, Yamaguchi, ’96; ...] [... ; Covi, Kim, Roszkowski, ’99; ...]

10

!6

10

!4

10

!2

10

4

10

5

10

6

10

7

10

8

10

9

CDM ←(m˜

a, TR)≈(100 keV, 106 GeV)

HDM ←(m˜

a, TR)≈(100 eV , 109 GeV)

[ ... ; Brandenburg, FDS, ’04]

a a

a

[Brandenburg, FDS, ‘04]

see also [Covi et al., ’01]

identical to the gravitino case

and [Strumia, ’10]

[Freitas, FDS, Tajuddin, Wyler, ’09]

slide-43
SLIDE 43

Steffen Axions etc. 39

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axino/ Gravitino Production

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?), ...

  • [Covi, Kim, Roszkowski, ’99]

freeze out m/Tf ~ 20

eq.

NLSP T < 10 GeV NLSP ! LSP + SM

10 GeV

WIMP freeze

  • ut

Gravitino Dark Matter

slide-44
SLIDE 44

Steffen Axions etc. 40

Stable Gravitino LSP

  • Thermal Leptogenesis

TR

  • [Pradler, FDS, ’07]

+ BBN constraints

CMSSM

[Pradler, FDS, arXiv:0710.2213]

TR 4.9 × 107 GeV

  • m e

G

10 GeV 1/5

BBN constraints

[Kohri, Moroi, Yotsuyanagi, ’05]

ΩDM constraint for gravitino DM + ΩDM constraint for neutralino DM

Unstable Gravitino

Thermal Leptogenesis requires T >109 GeV

Thermal Leptogenesis

Upper Limits on the Reheating Temperature TR

slide-45
SLIDE 45

Steffen Axions etc. 41

High Reheating Temperature Scenarios

BBN constraints

68% 27% 5%

standard particles

  • e

+ e τ decay analysis: m

ga gb gc a gc

e G

radiation dominated

  • mat. dom.

Λ dom. today 1eV 1 MeV inflation

? TR= 109 GeV ?

time Thermal EWIP production Thermal Leptogenesis

EWIP

∝ (p/MPl)n ∝ (TR/MPl)n

requires TR > 109 GeV ➔ baryon asymmetry

dark matter

stable & non-relativ. unstable

Big Bang Nucleosynthesis reheating temperature

slide-46
SLIDE 46

Steffen Axions etc. 42

  • Radiation content of the Universe at BBN and later
  • More radiation ! faster expansion ! more efficient BBN of 4He
  • More radiation ! later mat-rad eq ! visible in CMB + LSS

ρrad = ⇤ 1 + 7 8 (Nν + ∆Neff) T Tν ⇥4⌅ ργ

number of neutrinos neutrino temperature photon energy density

Parametrizes contribution of additional relativistic species

Data p.m./mean upper limit Y IT

p

+ [D/H]p 0.76 < 1.97 (3σ) Y Av

p

+ [D/H]p 0.77 < 3.53 (3σ) CMB + HPS + HST 1.73 < 3.59 (2σ)

BBN CMB + LSS

[Graf,Steffen; arXiv:1208.2951]

}

[Hamann et al.;’10]

Dark Radiation

constant H0 are taken into account. Data p.m./mean upper limit Y IT

p

[1] + [D/H]p [49] 0.76 < 1.97 (3σ) Y Av

p

[2] + [D/H]p [49] 0.77 < 3.53 (3σ) CMB + HPS + HST [6] 1.73 < 3.59 (2σ) Planck+WP+highL+BAO [8] 0.25 < 0.79 (2σ) Planck+WP+highL+H0+BAO [8] 0.47 < 0.95 (2σ)

BBN CMB + LSS

slide-47
SLIDE 47

Steffen Axions etc. 43

500 1000 1500 2000 1000 2000 3000 4000 5000 6000 7000 Delta Delta Delta ∆Neff = 0 ∆Neff = 1 ∆Neff = 2

l(l + 1)Cl/2π (µK2) l

6Li/H

N

7Li/H 7Be/H 3He/H

T/H D/H Yp H

SBBN f.o. D b.n. e± ann. n/p dec. ν dec. t/sec T/keV 0.1 1 10 100 1000 104 105 106 1000 100 10 1 1 10−2 10−4 10−6 10−8 10−10 10−12 10−14 SBBN f.o. D b.n. e± ann. n/p dec. ν dec. T/keV 1000 100 10 1 1 10−2 10−4 10−6 10−8 10−10 10−12 10−14

BBN CMB + LSS

slide-48
SLIDE 48

Steffen Axions etc. 44

Planck 2013 results XVI: Cosmological Parameters

D

at a given multipole. Combining Planck, WMAP polarization and the high-` experiments gives Neff = 3.36+0.68

−0.64

(95%; Planck+WP+highL). (74) The marginalized posterior distribution is given in Fig. 27 (black curve). Increasing Neff at fixed ✓∗ and zeq necessarily raises the ex- pansion rate at low redshifts too. Combining CMB with distance measurements can therefore improve constraints (see Fig. 27) al- though for the BAO observable rdrag/DV(z) the reduction in both rdrag and DV(z) with increasing Neff partly cancel. With the BAO data of Sect. 5.2, the Neff constraint is tightened to Neff = 3.30+0.54

−0.51

(95%; Planck+WP+highL+BAO). (75) Our constraints from CMB alone and CMB+BAO are compati- ble with the standard value Neff = 3.046 at the 1 level, giving no evidence for extra relativistic degrees of freedom. Since Neff is positively correlated with H0, the tension be- tween the Planck data and direct measurements of H0 in the base ΛCDM model (Sect. 5.3) can be reduced at the expense of high

  • Neff. The marginalized constraint is

Neff = 3.62+0.50

−0.48

(95%; Planck+WP+highL+H0). (76) For this data combination, the 2 for the best-fitting model al- lowing Neff to vary is lower by 5.0 than for the base Neff = 3.046

  • model. The H0 fit is much better, with ∆2 = −4.0, but there

is no strong preference either way from the CMB. The low-` temperature power spectrum does mildly favour the high Neff model (∆2 = −1.6) since Neff is positively correlated with ns (see Fig. 24) and increasing ns reduces power on large scales. The rest of the Planck power spectrum is agnostic (∆2 = −0.5), while the high-` experiments mildly disfavour high Neff in our fits (∆2 = 1.3). Further including the BAO data pulls the cen- tral value downwards by around 0.5 (see Fig. 27): Neff = 3.52+0.48

−0.45

(95%; Planck+WP+highL+H0+BAO). (77) The 2 at the best-fit for this data combination (Neff = 3.37) is lower by 3.6 than the best-fitting Neff = 3.046 model. While the high Neff best-fit is preferred by Planck+WP (∆2 = −3.3) and the H0 data (∆2 = −2.8 giving an acceptable 2 = 2.4 for this data point), it is disfavoured by the high-` CMB data (∆2 = 2.0) and slightly by BAO (∆2 = 0.4). We conclude that the tension between direct H0 measurements and the CMB and BAO data in the base ΛCDM can be relieved at the cost of additional neutrino-like physics, but there is no strong preference for this extension from the CMB damping tail. Throughout this subsection, we have assumed that all the

[Planck Collaboration, 1303.5076]

∆Neff = 3.62 + 0.5 - 3.046 = 1.074 @ 95% CL

slide-49
SLIDE 49

Steffen Axions etc. 45

Dark Radiation ➜ SUSY + PQ

[Graf, FDS, ’12]

  • Axions from decays of thermal saxions ! extra radiation
  • Calculation of thermally produced saxion yield done in a

gauge-invariant way

  • reheating temperature

Peccei Quinn scale strong coupling constant number density entropy density

saxion axion axion

Y TP

σ

⇥ 1.33 10−3g6

s ln

1.01 gs ⇥1011 GeV fPQ ⇥

2

TR 108 GeV ⇥

∆Neff ∝ 100 GeV mσ ⇥

1/2

fPQ 1011 GeV ⇥⇤ Y eq/TP

σ

10−3 ⌅ Lkin

PQ =

1 + p 2x vPQ σ ! 

⇥ 1 2∂µa∂µa + 1 2∂µσ∂µσ + i¯ ˜ aγµ∂µ˜ a

  • + . . .

p 2vPQ For m

a fPQ =

um expectation valu s vPQ = pP

i v2 i q2 i

x = X

i

q3

i v2 i

v2

PQ

.

slide-50
SLIDE 50

Steffen Axions etc. 46

High Reheating Temperature Scenarios

BBN constraints

68% 27% 5%

standard particles

  • e

+ e τ decay analysis: m

ga gb gc a gc

e G

radiation dominated

  • mat. dom.

Λ dom. today 1eV 1 MeV inflation

? TR= 109 GeV ?

time Thermal EWIP production Thermal Leptogenesis

EWIP

∝ (p/MPl)n ∝ (TR/MPl)n

requires TR > 109 GeV ➔ baryon asymmetry

dark matter

stable & non-relativ. unstable or relativ.

dark radiation

unstable

Big Bang Nucleosynthesis reheating temperature

slide-51
SLIDE 51

Steffen Axions etc. 47

Gravitino Dark Matter Scenario

  • Gravitino is the stable LSP (R-parity conservation is assumed)
  • Axino is heavy & unstable (decays prior to LOSP decoupling)
  • Saxion decays into axion dark radiation
  • Axion contributes to dark radiation and dark matter
  • Sneutrino NLSP case allows for thermal leptogenesis
slide-52
SLIDE 52

Steffen Axions etc. 48

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axino/ Gravitino Production

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?), ...

  • [Covi, Kim, Roszkowski, ’99]

freeze out m/Tf ~ 20

eq.

NLSP T < 10 GeV NLSP ! LSP + SM

10 GeV

WIMP freeze

  • ut

Gravitino Dark Matter

slide-53
SLIDE 53

Steffen Axions etc. 49

10

  • 10

10

  • 8

10

  • 6

10

  • 4

10

  • 2

10

8

10

9

10

10

10

11

10

12

R3ρrad S R

3

ρ

˜ a

R3ρσ R3ρa x = 1 x = 0.02

c c

mσ = 100 GeV TR = 109 GeV m˜

a = 6 TeV

m˜

g = 1 TeV

fPQ = 1011 GeV Ri = 1 GeV−1 ti = 1.6 × 10−13 s

t [s] R3ρ [GeV], S (a)

saxion ➞ 2 axions saxion ➞ 2 gluons axino ➞ gluon + gluino

Gravitino Dark Matter Scenario

[Graf, FDS, 1302.2143]

axino ➞ axion + gravitino

L e

G˜ aa = 1

2

  • ∂µσΨMνγµγν¯

˜ aM + i∂µaΨMνγµγνγ5˜ aM

slide-54
SLIDE 54

Steffen Axions etc. 50 10 100 10

8

10

9

10

10

  • mega

d = 0.79 d = 0.47 d = 0.25

m

1 / 2

= 400 GeV m

1 / 2

= 500 GeV m˜

g =1 TeV

m˜

g =1.25 TeV

c c

e G LSP me

a = 6 TeV

x = 1 fPQ = 1011 GeV ∆Neff = 0.25 ∆Neff = 0.47 ∆Neff = 0.79 Ω e

Gh2 = 0.124

m e

G = mσ [GeV]

TR [GeV]

(c)

Gravitino Dark Matter Scenario

slide-55
SLIDE 55

Steffen Axions etc. 51

[Pospelov, Pradler, FDS, ’08]

(C)BBN Constaints

disfavored by cosmological constraints

Gravitino LSP Case with a Charged Slepton NLSP

slide-56
SLIDE 56

Steffen Axions etc.

Particle Physics Cosmology

  • 2016: Large Hadron Collider (14 TeV)

sneutrino discovery at ATLAS & CMS

  • Intrinsic fine tuning problems

? Hierarchy Problem (mH << MPlanck)

? Strong CP Problem (ΘQCD << 1) ? Small Neutrino Masses (mν << mH)

mH = 125 GeV

68% 27% 5%

Standard particles dark energy

gravitino EWIP dark matter

  • 2013: Planck sky map
  • f the CMB radiation
  • Cosmological puzzles

? Matter-Antimatter Asymmetry

? Particle Identity & Origin of Dark Matter ? Dark Energy = Cosmological Constant

ESA

msneutrino = 415 GeV

thermal leptogenesis

✔ ✔

thermally produced gravitinos

✔ ✔

supersymmetry Peccei-Quinn symmetry

✔

See-saw mechanism

?

28

slide-57
SLIDE 57

Steffen Axions etc. 53

Axion Dark Matter Scenario

  • Axino is a very light stable LSP (R-parity conservation)
  • Gravitino is the NLSP and decays into axion & axino dark radiation
  • Saxion decays into axion dark radiation
  • Axion contributes to dark radiation and dark matter
  • Stau NLSP case & thermal leptogenesis is possible
slide-58
SLIDE 58

Steffen Axions etc. 54

t T

radiation dominated

  • mat. dom. Λ dom.

ρrad∝ a-4 ρmat∝ a-3 ρΛ∝ a0

t0=14 Gy T0=2.73 K

1eV 1 MeV 1s

100.000 y BBN LHC

inflation

slow roll reheat phase ρϕ∝ a0

V

  • 75%

20% 5%

Standard Model particles dark energy dark matter

a

TR= ?

reheating temp.

1 GeV

CνB CMB

e τ prod. at colliders (LHC, ILC, ...) + e τ collection + e τ decay analysis: m e

G, MPl (?),

+ ga gb gc a gc

e G

...

Very Early Hot Universe

T ~ 107 GeV

Thermal Axion Production

a

gb ga a gc

)

Axion Condensate

Axion Dark Matter

slide-59
SLIDE 59

Steffen Axions etc. 55

Lee-Weinberg Curve for Axions

[Graf, Steffen, ’12]

10

8

10

9

10

10

10

11

10

12

10

  • 10

10

  • 8

10

  • 6

10

  • 4

10

  • 2

1

∆Neff = 0.26 ∆Neff = 1.73 ∆Neff = 3.59

ΩCDMh2

θi = 1 θi = . 1 θi = . 1 TR = 1010 GeV TR = 108 GeV

c c c

ΩMIS

a

h2 ΩNTP

a

h2 Ωeq/TP

a

h2

fPQ [GeV] Ωah2

≥ Three Axion Populations

Axion Condensate: CDM

y ΩMIS

a

h2 ∼ 0.15 θ2

i (fPQ/1012 GeV)7/6

[... ; Sikivie, ’08; Kim, Carosi, ’08; ...]

slide-60
SLIDE 60

Steffen Axions etc. 56

saxion ➞ 2 axions saxion ➞ 2 gluons gravitino ➞ axion + axino

Axion Dark Matter Scenario

[Graf, FDS, 1302.2143]

10

  • 8

10

  • 5

10

  • 2

10 10

4

10

7

10

10

10 10

3

10

5

10

7

10

9

10

11

R3ρrad R3ρσ R3ρ e

G

R3ρdr

x = 1 x = 0.02

c c

mσ = m e

G = 100 GeV

TR = 5 × 109 GeV fPQ = 1012 GeV m1/2 = 400 GeV m˜

a < 37 eV

Ri = 1 GeV−1 ti = 1.6 × 10−13 s

t [s] R3ρ [GeV] (a) L e

G˜ aa = 1

2

  • ∂µσΨMνγµγν¯

˜ aM + i∂µaΨMνγµγνγ5˜ aM

slide-61
SLIDE 61

Steffen Axions etc. 57

100 1000 10

8

10

9

10

10

10

11

10

12

DeltaS DeltaG DeltaG JH

τ ˜

G = 5.2 × 1010 s

∆Neff = 0.78 ∆Neff = 3.59

400 GeV m1/2 = 600 GeV 400 GeV 600 GeV

  • a LSP,

G NLSP fPQ = 1012 GeV m˜

a < 37 eV

x = 1

∆N

G→˜ aa eff

+ ∆N σ→aa

eff

∆N

G→˜ aa eff

∆N

G→˜ aa eff

[JH,’12]

c c c c

m

G = mσ [GeV]

TR [GeV] (a)

b e f

  • r

e P l a n c k a f t e r P l a n c k

[Graf, Steffen,1302.2143]

Collider searches

Axion Dark Matter Scenario

slide-62
SLIDE 62

Steffen Axions etc. 58

|eQ| = 1/3 m2

˜ a/m2 ˜ τ 1

m ˜

B = 1.1 m˜ τ

m˜

τ = 300 GeV

Y˜

τ = 0.21 × 10−12

m ˜

G[GeV]

fa[GeV]

1 10 100 1012 1013 1014 1015 1016

106 s 104 s 1

2

s

Dsev

em

Dcons

em 3He/D 6Li

c

9Be

Γ2b

˜ a = x Γ˜ τ,2b tot

x = 0.01 x = 0.5 x = 0.99

|eQ| = 1/3 m ˜

B = 1.1 m˜ τ

m˜

τ = 1 TeV

m2

˜ a/m2 ˜ τ 1

Y˜

τ = 0.7 × 10−12

m ˜

G[GeV]

fa[GeV]

10 100 1000 1012 1013 1014 1015 1016

106 s 104 s 102 s

Dsev

had

Dsev

had

Dsev

em

Dcons

em 3He/D 6Li

c

9Be

Γ2b

˜ a = x Γ˜ τ,2b tot

x = 0.01 x = 0.5 x = 0.99

maxino, mgravitino < mstau

[Freitas, Tajuddin, FDS, Wyler, ’09]

slide-63
SLIDE 63

Steffen Axions etc. 59

mass 1 TeV 100 GeV gluino squark stau axino

a

~

100 1000 10

8

10

9

10

10

10

11

10

12

DeltaS DeltaG DeltaG JH

τ ˜

G = 5.2 × 1010 s

∆Neff = 0.78 ∆Neff = 3.59

400 GeV m1/2 = 600 GeV 400 GeV 600 GeV

  • a LSP,

G NLSP fPQ = 1012 GeV m˜

a < 37 eV

x = 1

∆N

G→˜ aa eff

+ ∆N σ→aa

eff

∆N

G→˜ aa eff

∆N

G→˜ aa eff

[JH,’12]

c c c c

m

G = mσ [GeV]

TR [GeV] (a)

b e f

  • r

e P l a n c k a f t e r P l a n c k

[Graf, Steffen,1302.2143]

Collider searches stau mass

LHC

2016

CHAMP

late decay

EWIP

Axion Dark Matter Scenario

slide-64
SLIDE 64

Steffen Axions etc.

Key questions on CHAMP properties Stable? Lifetime? Decay products? New detector concepts ➔ stop/collect CHAMPs ➔ study CHAMP decays

stau stau additional detector material

ILC

electron positron axino

tau

particle detector 20??

tau photon

axino

EWIP

EWIP

ILC

20??

proton proton stau stau

particle detector LHC 2009 LHC

2016

CHAMP CHAMP

12 60

☺ CHArged Massive Particles (CHAMPs) ☺

slide-65
SLIDE 65

Steffen Axions etc.

Particle Physics Cosmology

  • 2016: Large Hadron Collider (14 TeV)

stau discovery at ATLAS & CMS

  • Intrinsic fine tuning problems

? Hierarchy Problem (mH << MPlanck)

? Strong CP Problem (ΘQCD << 1) ? Small Neutrino Masses (mν << mH)

mH = 125 GeV

68% 27% 5%

Standard particles dark energy

axion EWIP dark matter

  • 2013: Planck sky map
  • f the CMB radiation
  • Cosmological puzzles

? Matter-Antimatter Asymmetry

? Particle Identity & Origin of Dark Matter ? Dark Energy = Cosmological Constant

ESA

mstau = 415 GeV

thermal leptogenesis

✔ ✔

axion condensate

✔ ✔

supersymmetry Peccei-Quinn symmetry

✔

See-saw mechanism

?

28 61

slide-66
SLIDE 66

Steffen Axions etc. 62

  • Cosmological observations still call for new physics
  • Hierachy problem & strong CP problem ➔ SUSY axion models
  • EWIPs are a new well-motivated class of particles
  • EWIP can explain dark matter and dark radiation (?)
  • High-reheating temperature scenarios ➔ thermal leptogenesis

➔ Gravitino dark matter with sneutino LOSPs ➔ Axion dark matter with stau LOSPs

  • Various cosmological aspects & promising collider propects

Conclusions